Suchergebnisse

Acknowledgements. We thank the referee Eric Emsellem for his detailed comments which helped to improve the content and presentation of the article. We thank the director of CEFCA, Dr. M. Moles, for his sincere support to this project. We thank the Viabilidad, Diseno, Acceso y Mejora funding program, ICTS-2009-10, and the Plan Nacional de Investigación y Desarrollo funding program, AYA2010-22111-C03-03, of the Spanish Ministerio de Ciencia e Innovacion, for the support given to this project. I.M. and J.M. acknowledge financial support from the Spanish grant AYA2010-15169 and Junta de Andalucía TIC114 and Excellence Project P08-TIC-03531. C.K., as a Humboldt Fellow, acknowledges support from the Alexander von Humboldt Foundation, Germany. B. Jungwiert acknowledges support by the grants AV0Z10030501 (Academy of Sciences of the Czech Republic) and LC06014 (Center for Theoretical Astrophysics, Czech Ministry of Education). T. Bartáková acknowledges support by the grants No. 205/08/H005 (Czech Science Foundation) and MUNI/A/0968/2009 (Masaryk University in Brno). Polychronis Papaderos is supported by a Ciencia 2008 contract, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). This paper makes use of the Sloan Digital Sky Survey data. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-PlanckInstitute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. ; The final product of galaxy evolution through cosmic time is the population of galaxies in the local universe. These galaxies are also those that can be studied in most detail, thus providing a stringent benchmark for our understanding of galaxy evolution. Through the huge success of spectroscopic single-fiber, statistical surveys of the Local Universe in the last decade, it has become clear, however, that an authoritative observational description of galaxies will involve measuring their spatially resolved properties over their full optical extent for a statistically significant sample. We present here the Calar Alto Legacy Integral Field Area (CALIFA) survey, which has been designed to provide a first step in this direction. We summarize the survey goals and design, including sample selection and observational strategy. We also showcase the data taken during the first observing runs (June/July 2010) and outline the reduction pipeline, quality control schemes and general characteristics of the reduced data. This survey is obtaining spatially resolved spectroscopic information of a diameter selected sample of ~600 galaxies in the Local Universe (0.005 < z < 0.03). CALIFA has been designed to allow the building of two-dimensional maps of the following quantities: (a) stellar populations: ages and metallicities; (b) ionized gas: distribution, excitation mechanism and chemical abundances; and (c) kinematic properties: both from stellar and ionized gas components. CALIFA uses the PPAK integral field unit (IFU), with a hexagonal field-of-view of ~1.3⎕′, with a 100% covering factor by adopting a three-pointing dithering scheme. The optical wavelength range is covered from 3700 to 7000 Å, using two overlapping setups (V500 and V1200), with different resolutions: R ~ 850 and R ~ 1650, respectively. CALIFA is a legacy survey, intended for the community. The reduced data will be released, once the quality has been guaranteed. The analyzed data fulfillthe expectations of the original observing proposal, on the basis of a set of quality checks and exploratory analysis: (i) the final datacubes reach a 3σ limiting surface brightness depth of ~23.0 mag/arcsec2 for the V500 grating data (~22.8 mag/arcsec2 for V1200); (ii) about ~70% of the covered field-of-view is above this 3σ limit; (iii) the data have a blue-to-red relative flux calibration within a few percent in most of the wavelength range; (iv) the absolute flux calibration is accurate within ~8%with respect to SDSS; (v) the measured spectral resolution is ~85 km s-1 for V1200 (~150 km s-1 for V500); (vi) the estimated accuracy of the wavelength calibration is ~5 km s-1 for the V1200 data (~10 km s-1 for the V500 data); (vii) the aperture matched CALIFA and SDSS spectra are qualitatively and quantitatively similar. Finally, we show that we are able to carry out all measurements indicated above, recovering the properties of the stellar populations, the ionized gas andthe kinematics of both components. The associated maps illustrate the spatial variation of these parameters across the field, reemphasizing the redshift dependence of single aperture spectroscopic measurements. We conclude from this first look at the data that CALIFA will be an important resource for archaeological studies of galaxies in the Local Universe. ; CEFCA ; Viabilidad, Diseno, Acceso y Mejora ICTS-2009-10 ; Instituto de Salud Carlos III Spanish Government AYA2010-22111-C03-03 ; Spanish grant AYA2010-15169 ; Junta de Andalucia TIC114 ; Excellence Project P08-TIC-03531 ; Alexander von Humboldt Foundation ; Czech Academy of Sciences AV0Z10030501 ; Center for Theoretical Astrophysics, Czech Ministry of Education LC06014 ; Grant Agency of the Czech Republic 205/08/H005 ; Masaryk University in Brno MUNI/A/0968/2009 ; Ciencia 2008 contract ; Portuguese Foundation for Science and Technology ; European Commission Joint Research Centre ; European Social Fund (ESF) ; Alfred P. Sloan Foundation ; National Science Foundation (NSF) ; United States Department of Energy (DOE) ; National Aeronautics & Space Administration (NASA) ; Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) ; Max Planck Society Foundation CELLEX ; Higher Education Funding Council for England ; Science & Technology Facilities Council (STFC) ST/H00243X/1 ST/J001538/1 ST/H004912/1

AT2018cow was the nearest and best studied example of a new breed of extra-galactic, luminous and rapidly-evolving transient. Both the progenitor systems and explosion mechanisms of these rapid transients remain a mystery { the energetics, spectral signa- tures, and timescales make them challenging to interpret in established classes of super- novae and tidal disruption events. The rich, multi-wavelength data-set of AT2018cow has still left several interpretations viable to explain the nature of this event. In this paper we analyse integral- eld spectroscopic data of the host galaxy, CGCG137-068, to compare environmental constraints with leading progenitor models. We nd the explosion site of AT2018cow to be very typical of core-collapse supernovae (known to form from stars with MZAMS 8-25 M ), and infer a young stellar population age at the explosion site of few 10Myr, at slightly sub-solar metallicity. When comparing to expectations for exotic intermediate-mass black hole (IMBH) tidal disruption events, we nd no evidence for a potential host system of the IMBH. In particular, there are no abrupt changes in metallicity or kinematics in the vicinity of the explosion site, ar- guing against the presence of a distinct host system. The proximity of AT2018cow to strong star-formation in the host galaxy makes us favour a massive stellar progenitor for this event. ; Science & Technology Facilities Council (STFC) Science and Technology Development Fund (STDF) ST/P000495/1 ; European Union (EU) 839090 ; European Union (EU) PGC2018-095317-B-C21 ; Consejo Nacional de Ciencia y Tecnologia (CONACyT) CB-285080 FC-2016-01-1916 ; (UNAM) project PAPIIT-DGAPA-IN100519 ; European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 0103.D-0440(A)

We present a novel method to retrieve the chemical structure of galaxies using integral field spectroscopy data through the stellar Metallicity Distribution Function (MDF). This is the probability distribution of observing stellar populations having a metallicity Z. We apply this method to a set of 550 galaxies from the CALIFA survey. We present the behaviour of the MDF as a function of the morphology, the stellar mass, and the radial distance. We use the stellar metallicity radial profiles retrieved as the first moment of the MDF, as an internal test for our method. The gradients in these radial profiles are consistent with the known trends: they are negative in massive early-type galaxies and tend to positive values in less massive late-type ones. We find that these radial profiles may not convey the complex chemical structure of some galaxy types. Overall, low mass galaxies (log M·/M· ≤ 10) have broad MDFs (σZ∼ 1.0 dex), with unclear dependence on their morphology. However this result is likely affected by under-represented bins in our sample. On the other hand, massive galaxies (log M·/M· ≥ 11) have systematically narrower MDFs (σZ≤ 0.2 dex). We find a clear trend whereby the MDFs at rk/Re > 1.5 have large variance. This result is consistent with sparse SFHs in medium/low stellar density regions. We further find there are multimodal MDFs in the outskirts (∼ 18%) and the central regions (∼ 40%) of galaxies. This behaviour is linked to a fast chemical enrichment during early stages of the SFH, along with the posterior formation of a metal-poor stellar population. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. ; We thank CONACYT FC-2016-01-1916 and CB-285080 projects and PAPIIT IN100519 project for support on this study. AMN specially thanks Carlos López-Cobá who selflessly shared his calculation of isophotal parameters for the sample used in this paper. AMN also thanks Jorge Barrera-Ballesteros for useful comments that improved an early version of this paper. AMN and EADL thank all Stellar Population Synthesis and Chemical Evolution group of the Instituto de Astronomía – UNAM for the help through the by-eye morphological classification. LG was funded by the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 839090. RGB acknowledges support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). ; Peer reviewed

We present a new catalogue of H ii regions based on the integral field spectroscopy (IFS) data of the extended CALIFA and PISCO samples. The selection of H ii regions was based on two assumptions: a clumpy structure with high contrast of H α emission and an underlying stellar population comprising young stars. The catalogue provides the spectroscopic information of 26 408 individual regions corresponding to 924 galaxies, including the flux intensities and equivalent widths of 51 emission lines covering the wavelength range between 3745 and 7200 Å. To our knowledge, this is the largest catalogue of spectroscopic properties of H ii regions. We explore a new approach to decontaminate the emission lines from diffuse ionized gas contribution. This diffuse gas correction was estimated to correct every emission line within the considered spectral range. With the catalogue of H ii regions corrected, new demarcation lines are proposed for the classical diagnostic diagrams. Finally, we study the properties of the underlying stellar populations of the H ii regions. It was found that there is a direct relationship between the ionization conditions on the nebulae and the properties of stellar populations besides the physicals condition on the ionized regions.© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society ; We thank the referee for the helpful comments that have improved the quality of this article. We are grateful for the support of CONACYT grants CB-285080, FC-2016-01-1916, and CB2015-254132, and funding from the DGAPA/PAPIIT-IA101217, DGAPA/PAPIITIN100519, and DGAPA/PAPIIT-107215 (UNAM) projects. This study uses data provided by the CALIFA survey (http://ca lifa.caha.es/); it is based on observations collected at the Centro Astronomico Hispano Alem ´ an (CAHA) at Calar Alto, operated ´ jointly by the Max-Planck-Institut fur Astronomie and the Instituto ¨ de Astrof´ısica de Andaluc´ıa (CSIC). LG was funded by the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 839090. This research makes use of python (http://www.python.org), of Matplotlib (a framework to the creation of scientific plots for Python; Hunter 2007), Astropy (a Python package for astronomy; Astropy Collaboration 2013; Price-Whelan et al. 2018), and SciPy (a Python-based ecosystem of open-source software for mathematics, science, and engineering; Jones et al. 2001). ; Peer reviewed

We characterised the oxygen abundance radial distribution of a sample of 102 spiral galaxies observed with VLT/MUSE using the O3N2 calibrator. The high spatial resolution of the data allowed us to detect 14345 H ii regions with the same image quality as with photometric data, avoiding any dilution effect. We developed a new methodology to automatically fit the abundance radial profiles, finding that 55 galaxies of the sample exhibit a single negative gradient. The remaining 47 galaxies also display, as well as this negative trend, either an inner drop in the abundances (21), an outer flattening (10), or both (16), which suggests that these features are a common property of disc galaxies. The presence and depth of the inner drop depends on the stellar mass of the galaxies with the most massive systems presenting the deepest abundance drops, while there is no such dependence in the case of the outer flattening. We find that the inner drop appears always around 0.5 r, while the position of the outer flattening varies over a wide range of galactocentric distances. Regarding the main negative gradient, we find a characteristic slope in the sample of α =-0.10 ± 0.03 dex /r. This slope is independent of the presence of bars and the density of the environment. However, when inner drops or outer flattenings are detected, slightly steeper gradients are observed. This suggests that radial motions might play an important role in shaping the abundance profiles. We define a new normalisation scale (>the abundance scale length>, r) for the radial profiles based on the characteristic abundance gradient, with which all the galaxies show a similar position for the inner drop (~0.5 r) and the outer flattening (~1.5 r). Finally, we find no significant dependence of the dispersion around the negative gradient with any property of the galaxies, with values compatible with the uncertainties associated with the derivation of the abundances.© ESO, 2018. ; This study is based on observations made with ESO Telescopes at the Paranal Observatory (programmes 60.A-9329(A), 095.D-0172(A), 95.D-0091(A), 95.D-0091(B), 096.D-0263(A), 96.D-0296(A), 97.D-0408(A) and 98.D-0115(A)) and has also made use of the services of the ESO Science Archive Facility (programmes 60.A-9319(A), 60.A-9100(B), 60.A-9329(A), 60.A-9339(A), 60.A-9301(A), 196.B-0578(A) and 094.B-0733(B)). We would like to thank the anonymous referee for comments which helped to improve the content of the paper. We acknowledge financial support from the Spanish Ministerio de Economia y Competitividad (MINECO) via grants AYA2012-31935, and from the >Junta de Andalucia> local government through the FQM-108 project. We also acknowledge support to the ConaCyt funding programme 180125 and DGAPA IA100815. L.G. is supported in part by the US National Science Foundation under Grant AST-1311862. T.K. acknowledges support through the Sofja Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation of Germany. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr).This research also makes use of python (http://www.python.org),of Matplotlib (Hunter 2007), a suite of open-source python modules that provides a framework for creating scientific plots, and Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013).

NGC 7469 is a well-known luminous infrared galaxy, with a circumnuclear star formation ring ∼830 pc radius) surrounding a Seyfert 1 active galactic nucleus (AGN). Nuclear unresolved winds were previously detected in X-rays and ultraviolet, as well as an extended biconical outflow in infrared coronal lines. We search for extended outflows by measuring the kinematics of the Hβ and [O III] λ5007 optical emission lines, in data of the Very Large Telescope/Multi-unit Spectroscopic Explorer integral field spectrograph. We find evidence of two outflow kinematic regimes: One slower regime extending across most of the star formation (SF) ring-possibly driven by the massive SF-and a faster regime (with a maximum velocity of -715 km s-1), only observed in [O III], in the western region between the AGN and the massive star-forming regions of the ring, likely AGN-driven. This work shows a case where combined AGN/SF feedback can be effectively spatially resolved, opening up a promising path toward a deeper understanding of feedback processes in the central kiloparsec of AGN ; Support from CONACyT (Mexico) grant CB-2016-01-286316 is acknowledged. J.P.T.P. acknowledges DAIP-UGto (Mexico) for granted support (0173/2019). Y.A. acknowledges support from project PID2019-107408GB-C42 (Ministerio de Ciencia e Innovación, Spain). S.F.S. thanks the support of CONACYT grants CB-285080 and FC-2016-01- 1916, and funding from the PAPIIT-DGAPA-IN100519 (UNAM) project. L.G. was funded by the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). E.B acknowledges the support from Comunidad de Madrid through the Atracción de Talento grant 2017-T1/TIC-5213. This research has been partially funded by the Spanish State Research Agency (AEI) Project MDM-2017-0737 Unidad de Excelencia "María de Maeztu"- Centro de Astrobiología (INTA-CSIC)

Astronomy & Astrophysics 587 (2016): A70 reproduced with permission from Astronomy & Astrophysics ; We measured the gas abundance profiles in a sample of 122 face-on spiral galaxies observed by the CALIFA survey and included all spaxels whose line emission was consistent with star formation. This type of analysis allowed us to improve the statistics with respect to previous studies, and to properly estimate the oxygen distribution across the entire disc to a distance of up to 3-4 disc effective radii (re). We confirm the results obtained from classical H ii region analysis. In addition to the general negative gradient, an outer flattening can be observed in the oxygen abundance radial profile. An inner drop is also found in some cases. There is a common abundance gradient between 0.5 and 2.0 re of αO/H =-0.075 dex/re with a scatter of σ = 0.016 dex/re when normalising the distances to the disc effective radius. By performing a set of Kolmogorov-Smirnov tests, we determined that this slope is independent of other galaxy properties, such as morphology, absolute magnitude, and the presence or absence of bars. In particular, barred galaxies do not seem to display shallower gradients, as predicted by numerical simulations. Interestingly, we find that most of thegalaxies in the sample with reliable oxygen abundance values beyond ~2 effective radii (57 galaxies) present a flattening of the abundance gradient in these outer regions. This flattening is not associated with any morphological feature, which suggests that it is a common property of disc galaxies. Finally, we detect a drop or truncation of the abundance in the inner regions of 27 galaxies in the sample; this is only visible for the most massive galaxies ; We acknowledge financial support from the Spanish Ministerio de Economía y Competitividad (MINECO) via grant AYA2012-31935, and from the "Junta de Andalucía" local government through the FQM-108 project. We also acknowledge support to the ConaCyt funding program 180125. Y.A. acknowledges fi- nantial support from the Ramón y Cajal programme (RyC-2011-09461). Y.A. and A.I.D. acknowledge support from the project AYA2013-47742-C4-3-P from the Spanish MINECO, as well as the "Study of Emission-Line Galaxies with Integral-Field Spectroscopy" (SELGIFS) programme, funded by the EU (FP7- PEOPLE-2013-IRSES-612701). Support for L.G. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG acknowledges support by CONICYT through FONDECYT grant 3140566. R.M.G.D. acknowledges support from the Spanish grant AYA2014-57490-P, and from the "Junta de Andalucía" P12-FQM2828 project. RAM thanks the Spanish program of International Campus of Excellence Moncloa (CEI). IM and A.d.O. acknowledge support from the Spanish MINECO grant AYA2013-42227P. JMA acknowledges support from the European Research Council Starting Grant (SEDmorph, P.I. V. Wild). Support for MM has been provided by DGICYT grant AYA2013-47742-C4-4-P. PSB acknowledges support from the Ramón y Cajal programme, grant ATA2010-21322-C03-02 from the Spanish MINECO. CJW acknowledges support through the Marie Curie Career Grant Integration 303912

This paper describes the third public data release (DR3) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. Science-grade quality data for 667 galaxies are made public, including the 200 galaxies of the second public data release (DR2). Data were obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto Observatory. Three different spectral setups are available: i) a low-resolution V500 setup covering the wavelength range 3745-7500 Å (4240-7140 Å unvignetted) with a spectral resolution of 6.0 Å (FWHM) for 646 galaxies, ii) a medium-resolution V1200 setup covering the wavelength range 3650-4840 Å (3650-4620 Å unvignetted) with a spectral resolution of 2.3 Å (FWHM) for 484 galaxies, and iii) the combination of the cubes from both setups (called COMBO) with a spectral resolution of 6.0 Å and a wavelength range between 3700-7500 Å (3700-7140 Å unvignetted) for 446 galaxies. The Main Sample, selected and observed according to the CALIFA survey strategy covers a redshift range between 0.005 and 0.03, spans the color-magnitude diagram and probes a wide range of stellar masses, ionization conditions, and morphological types. The Extension Sample covers several types of galaxies that are rare in the overall galaxy population and are therefore not numerous or absent in the CALIFA Main Sample. All the cubes in the data release were processed using the latest pipeline, which includes improved versions of the calibration frames and an even further improved image reconstruction quality. In total, the third data release contains 1576 datacubes, including ~1.5 million independent spectra. ; Fil: Sánchez, S. F. Universidad Nacional Autónoma de México; México ; Fil: Garciá Benito, R. Instituto de Astrofísica de Andalucía; España ; Fil: Zibetti, S. Osservatorio Astrofisico di Arcetri; Italia ; Fil: Walcher, C. J. Leibniz-Institut für Astrophysik Potsdam; Alemania ; Fil: Husemann, B. European Southern Observatory; Alemania ; Fil: Mast, Damian. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina ; Fil: López Fernández, R. Instituto de Astrofísica de Andalucía; España ; Fil: López Sánchez, A. R. Sydney Institute for Astronomy; Australia ; Fil: Lyubenova, M. University of Groningen. Kapteyn Astronomical Institute; Países Bajos ; Fil: Marino, R. Institut für Astronomie; Suiza ; Fil: Márquez, I. Instituto de Astrofísica de Andalucía; España ; Fil: Mendez Abreu, J. University of St. Andrews. School of Physics and Astronomy; Reino Unido ; Fil: Mollá, M. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas; España ; Fil: Monreal Ibero, A. Université Paris Diderot. Observatoire de Paris; Francia ; Fil: Ortega Minakata, R. Universidade Federal do Rio de Janeiro. Observatorio do Valongo; Brasil ; Fil: Torres Papaqui, J. P. Universidad de Guanajuato. Departamento de Astronomía; México ; Fil: Pérez, E. Instituto de Astrofísica de Andalucía; España ; Fil: Rosales Ortega, F. F. Instituto Nacional de Astrofísica, Óptica y Electrónica; México ; Fil: Roth, M. M. Leibniz-Institut für Astrophysik Potsdam; Alemania ; Fil: Sánchez Blázquez, P. Universidad Autónoma de Madrid. Facultad de Ciencias. Departamento de Física Teórica; España ; Fil: Schilling, U. Ruhr-Universität Bochum. Astronomisches Institut; Alemania ; Fil: Spekkens, K. Royal Military College of Canada. Department of Physics; Canadá ; Fil: Vale Asari, N. Universidade Federal de Santa Catarina. Departamento de Física; Brasil ; Fil: Van Den Bosch, R. C. E. Max-Planck-Institut für Astronomie; Alemania ; Fil: Van De Ven, G. Max-Planck-Institut für Astronomie; Alemania ; Fil: Vilchez, J. M. Instituto de Astrofísica de Andalucía; España ; Fil: Wild, V. University of St. Andrews. School of Physics and Astronomy; Reino Unido ; Fil: Wisotzki, L. Leibniz-Institut für Astrophysik Potsdam; Alemania ; Fil: Ylldlrlm, A. Max-Planck-Institut für Astronomie; Alemania ; Fil: Ziegler, B. Department of Astrophysics. University of Vienna; Austria